A mass-dependent density profile for dark matter haloes including the influence of galaxy formation

Cintio, Arianna Di; Brook, Chris; Dutton, Aaron A.; Macciò, Andrea V.; Stinson, Greg; Knebe, Alexander

doi:10.1093/mnras/stu729

Cited by 295 publications

(458 citation statements)

References 85 publications

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“…On the other hand, SIDM with m 0.5 cm g Based on these results, an ideal scale to investigate possible DM self-interactions appears to be the dwarf galaxy scale with halo masses M 10 10 11 - scale, as they will have the largest interaction cross-sections and the least contracted halos. However, these are precisely the halos expected to be most vulnerable to stellar feedback Di Cintio et al 2014;Oñorbe et al 2015). Ongoing work (Vogelsberger et al 2014;Fry et al 2015;V.…”

Section: Discussionmentioning

confidence: 96%

“…SIDM cores also may provide a natural explanation for the unexpectedly low densities of local dwarf galaxies (Vogelsberger et al 2012(Vogelsberger et al , 2014Elbert et al 2015), which is a problem known as "Too Big to Fail" (TBTF; Boylan-Kolchin et al 2011Ferrero et al 2012;Garrison-Kimmel et al 2014;Tollerud et al 2014;Klypin et al 2015;Papastergis et al 2015). There are many in the galaxy formation community who believe these issues may be resolved by baryonic processes, such as supernova feedback (Navarro et al 1996;Read & Gilmore 2005;Governato et al 2012;Di Cintio et al 2014;Maxwell et al 2015;Oñorbe et al 2015;Dutton et al 2016;Read et al 2016;Katz et al 2017), though not all authors necessarily agree (Peñarrubia et al 2012;Garrison-Kimmel et al 2013;Pace 2016). Tidal effects have been shown to solve TBTF in satellite galaxies (see e.g., Read et al 2006;Zolotov et al 2012;Arraki et al 2014;Brooks & Zolotov 2014;Del Popolo et al 2014), but the evidence for TBTF in the local field (Garrison-Kimmel et al 2014;Kirby et al 2014) necessitates another solution for these galaxies.…”

Section: Introductionmentioning

confidence: 99%

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A Testable Conspiracy: Simulating Baryonic Effects on Self-interacting Dark Matter Halos

Elbert

Bullock

Kaplinghat

et al. 2018

ApJ

111

116

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We investigate the response of self-interacting dark matter (SIDM) halos to the growth of galaxy potentials using idealized simulations, with each run in tandem with collisionless cold dark matter (CDM). We find that if the stellar potential strongly dominates in the central parts of a galaxy, then SIDM halos can be as dense as CDM halos on observable scales. For extreme cases, core collapse can occur, leading to SIDM halos that are denser and cuspier than their CDM counterparts. If the stellar potential is not dominant, then SIDM halos retain isothermal cores with densities far below CDM predictions. When a disk is present, the inner SIDM halo becomes more flattened in the disk plane than the CDM halo.  s -is disfavored for DM collision velocities above about 1500 km s −1 . More generally, the interaction between baryonic potentials and SIDM densities offers new directions for constraining SIDM cross-sections in galaxies where baryons are dynamically important.

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Section: Discussionmentioning

confidence: 96%

Section: Introductionmentioning

confidence: 99%

A Testable Conspiracy: Simulating Baryonic Effects on Self-interacting Dark Matter Halos

Elbert

Bullock

Kaplinghat

et al. 2018

ApJ

111

116

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“…In a ΛCDM model, one can relate the halo mass as inferred from the fit to the rotation curve to M b , and compare this relation to the M b -M halo relation that emerges from abundance matching studies. We will undertake such a procedure in a forthcoming study (Katz, H et al in prep), comparing a ΛCDM model that assumes an NFW profile (Navarro et al 1996) with a model where DM halo shapes are modified by baryons (Di Cintio et al 2014a). …”

Section: Discussionmentioning

confidence: 99%

The different baryonic Tully–Fisher relations at low masses

Santos-Santos

Stinson

2016

Mon. Not. R. Astron. Soc.

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We compare the Baryonic Tully-Fisher relation (BTFR) of simulations and observations of galaxies ranging from dwarfs to spirals, using various measures of rotational velocity V rot . We explore the BTFR when measuring V rot at the flat part of the rotation curve, V flat , at the extent of HI gas, V last , and using 20% (W 20 ) and 50% (W 50 ) of the width of HI line profiles. We also compare with the maximum circular velocity of the parent halo, V DM max , within dark matter only simulations. The different BTFRs increasingly diverge as galaxy mass decreases. Using V last one obtains a power law over four orders of magnitude in baryonic mass, with slope similar to the observed BTFR. Measuring V flat gives similar results as V last when galaxies with rising rotation curves are excluded. However, higher rotation velocities would be found for low mass galaxies if the cold gas extended far enough for V rot to reach a maximum. W 20 gives a similar slope as V last but with slightly lower values of V rot for low mass galaxies, although this may depend on the extent of the gas in your galaxy sample. W 50 bends away from these other relations toward low velocities at low masses. By contrast, V DM max bends toward high velocities for low mass galaxies, as cold gas does not extend out to the radius at which halos reach V DM max . Our study highlights the need for careful comparisons between observations and models: one needs to be consistent about the particular method of measuring V rot , and precise about the radius at which velocities are measured.

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“…For even higher efficiencies α increases, reaching the CDM value of α ≈ 1.2 at an efficiency of ∼ 20%, and steeper values as high as α ≈ 2 for efficiencies approaching unity. Di Cintio et al (2014b) present a parametrization of the dark matter density profiles in the MaGICC simulations , using a five parameter function. As with the inner slope, the other parameters were found to depend on ǫSF.…”

Section: Introductionmentioning

confidence: 99%

NIHAO IX: the role of gas inflows and outflows in driving the contraction and expansion of cold dark matter haloes

Dutton

Macciò

Dekel³

et al. 2016

Mon. Not. R. Astron. Soc.

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101

118

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We use ∼ 100 cosmological galaxy formation 'zoom-in' simulations using the smoothed particle hydrodynamics code gasoline to study the effect of baryonic processes on the mass profiles of cold dark matter haloes. The haloes in our study range from dwarf (M 200 ∼ 10 10 M ⊙ ) to Milky Way (M 200 ∼ 10 12 M ⊙ ) masses. Our simulations exhibit a wide range of halo responses, primarily varying with mass, from expansion to contraction, with up to factor ∼ 10 changes in the enclosed dark matter mass at 1 per cent of the virial radius. Confirming previous studies, the halo response is correlated with the integrated efficiency of star formation:In addition, we report a new correlation with the compactness of the stellar system: ǫ R ≡ r 1/2 /R 200 . We provide an analytic formula depending on ǫ SF and ǫ R for the response of cold dark matter haloes to baryonic processes. An observationally testable prediction is that, at fixed mass, larger galaxies experience more halo expansion, while the smaller galaxies more halo contraction. This diversity of dark halo response is captured by a toy model consisting of cycles of adiabatic inflow (causing contraction) and impulsive gas outflow (causing expansion). For net outflow, or equal inflow and outflow fractions, f , the overall effect is expansion, with more expansion with larger f . For net inflow, contraction occurs for small f (large radii), while expansion occurs for large f (small radii), recovering the phenomenology seen in our simulations. These regularities in the galaxy formation process provide a step towards a fully predictive model for the structure of cold dark matter haloes.

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A mass-dependent density profile for dark matter haloes including the influence of galaxy formation

Cited by 295 publications

References 85 publications

A Testable Conspiracy: Simulating Baryonic Effects on Self-interacting Dark Matter Halos

A Testable Conspiracy: Simulating Baryonic Effects on Self-interacting Dark Matter Halos

The different baryonic Tully–Fisher relations at low masses

NIHAO IX: the role of gas inflows and outflows in driving the contraction and expansion of cold dark matter haloes

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